  We continue our study of the spectral energy distributions (SEDs) of 11 AGN
at 1.5 < z < 2.2, with optical-NIR spectra, X-ray data and mid-IR photometry.
In a previous paper we presented the observations and models; in this paper we
explore the parameter space of these models. We first quantify uncertainties on
the black hole masses (M$_{\rm BH}$) and degeneracies between SED parameters.
The effect of BH spin is tested, and we find that while low to moderate spin
values (a$_*$ $\leq$ 0.9) are compatible with the data in all cases, maximal
spin (a$_*$ = 0.998) can only describe the data if the accretion disc is
face-on. The outer accretion disc radii are well constrained in 8/11 objects,
and are found to be a factor ~5 smaller than the self-gravity radii. We then
extend our modelling campaign into the mid-IR regime with WISE photometry,
adding components for the host galaxy and dusty torus. Our estimates of the
host galaxy luminosities are consistent with the M$_{\rm BH}$-bulge
relationship, and the measured torus properties (covering factor and
temperatures) are in agreement with earlier work, suggesting a predominantly
silicate-based grain composition. Finally, we deconvolve the optical-NIR
spectra using our SED continuum model. We claim that this is a more physically
motivated approach than using empirical descriptions of the continuum such as
broken power-laws. For our small sample, we verify previously noted
correlations between emission linewidths and luminosities commonly used for
single-epoch M$_{\rm BH}$ estimates, and observe a statistically significant
anti-correlation between [O III] equivalent width and AGN luminosity.
