Herron, C. A.Burkhart, BlakesleyGaensler, B. M.Lewis, Geraint FrancisMcClure-Griffiths, NaomiBernardi, GianniCarretti, EttoreHaverkorn, M.Kesteven, M. J.Poppi, SergioStaveley-Smith, Lister2021-04-220004-637Xhttp://hdl.handle.net/1885/230958Diagnostics of polarized emission provide us with valuable information on the Galactic magnetic field and the state of turbulence in the interstellar medium, which cannot be obtained from synchrotron intensity alone. In Paper I, we derived polarization diagnostics that are rotationally and translationally invariant in the Q-U plane, similar to the polarization gradient. In this paper, we apply these diagnostics to simulations of ideal magnetohydrodynamic turbulence that have a range of sonic and Alfvénic Mach numbers. We generate synthetic images of Stokes Q and U for these simulations for the cases where the turbulence is illuminated from behind by uniform polarized emission and where the polarized emission originates from within the turbulent volume. From these simulated images, we calculate the polarization diagnostics derived in Paper I for different lines of sight relative to the mean magnetic field and for a range of frequencies. For all of our simulations, we find that the polarization gradient is very similar to the generalized polarization gradient and that both trace spatial variations in the magnetoionic medium for the case where emission originates within the turbulent volume, provided that the medium is not supersonic. We propose a method for distinguishing the cases of emission coming from behind or within a turbulent, Faraday rotating medium and a method to partly map the rotation measure of the observed region. We also speculate on statistics of these diagnostics that may allow us to constrain the physical properties of an observed turbulent region.C.A.H. acknowledges financial support received via an Australian Postgraduate Award and a Vice Chancellor’s Research Scholarship awarded by the University of Sydney. B.B. is supported by the NASA Einstein Postdoctoral Fellowship. B.M.G. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) through grant RGPIN-2015-05948 and a Canada Research Chair. N.M.M.-G. acknowledges the support of the Australian Research Council through grant FT150100024. The Dunlap Institute for Astronomy and Astrophysics is funded through an endowment established by the David Dunlap family and the University of Toronto.application/pdfen-AU© 2018 The American Astronomical SocietyISM: magnetic fieldsISM: structuremagnetohydrodynamics (MHD)polarizationtechniques: polarimetric2018-03-0510.3847/1538-4357/aaafd02020-11-23