  Building on our first paper in this series, we investigate the impact of
radial magnetic fields and non-ideal magnetohydrodynamic (MHD) effects -
specifically, Ohmic resistivity, Hall drift, and ambipolar diffusion - on RWI
unstable modes. The presence of a radial field is linked to the disk's vertical
shear and vertical magnetic field. We perform radially global linear analyses
and utilize the spectral code \textsc{Dedalus} to solve the matrix eigenvalue
problems. Our findings reveal that radial fields exhibit behavior similar to
vertical fields. In the ideal MHD limit, radial fields enhance the effect of
vertical fields in reducing growth rates, with significant reductions starting
at relatively weak field strengths, around $\beta \sim 10^3 - 10^4$, which are
relevant to protoplanetary disks. In the non-ideal MHD limit, all three
non-ideal effects, when sufficiently strong, cause the growth rates to closely
resemble those observed in hydrodynamic models.
