  We present detailed observations of photoionization conditions and galaxy
kinematics in eleven z$=1.39-2.59$ radio-loud quasar host galaxies. Data was
taken with OSIRIS integral field spectrograph (IFS) and the adaptive optics
system at the W.M. Keck Observatory that targeted nebular emission lines
(H$\beta$,[OIII],H$\alpha$,[NII]) redshifted into the near-infrared (1-2.4
\micron). We detect extended ionized emission on scales ranging from 1-30 kpc
photoionized by stars, shocks, and active galactic nuclei (AGN). Spatially
resolved emission-line ratios indicate that our systems reside off the star
formation and AGN-mixing sequence on the Baldwin, Phillips $\&$ Terlevich (BPT)
diagram at low redshift. The dominant cause of the difference between line
ratios of low redshift galaxies and our sample is due to lower gas-phase
metallicities, which are 2-5$\times$ less compared to galaxies with AGN in the
nearby Universe. Using gas velocity dispersion as a proxy to stellar velocity
dispersion and dynamical mass measurement through inclined disk modeling we
find that the quasar host galaxies are under-massive relative to their central
supermassive black hole (SMBH) mass, with all systems residing off the local
scaling ($M_{\bullet}-\sigma~$,$M_{\bullet}-M_{*}~$) relationship. These quasar
host galaxies require substantial growth, up to an order of magnitude in
stellar mass, to grow into present-day massive elliptical galaxies. Combining
these results with part I of our sample paper (Vayner et al. 2021) we find
evidence for winds capable of causing feedback before the AGN host galaxies
land on the local scaling relation between black hole and galaxy stellar mass,
and before the enrichment of the ISM to a level observed in local galaxies with
AGN.
