  We present a comprehensive analysis of the post-outburst evolution of the FU
Ori object HBC 722 in optical/near-infrared (NIR) photometry and spectroscopy.
Using a modified viscous accretion disk model, we fit the outburst epoch SED to
determine the physical parameters of the disk, including $\dot{M}_\mathrm{acc}
= 10^{-4.0} \ M_\odot$ yr$^{-1}$, $R_\mathrm{inner} = 3.65 \ R_\odot$, $i =
79^\circ$, and a maximum disk temperature of $T_\mathrm{max} = 5700$ K. We then
use a decade of optical/NIR spectra to demonstrate a changing accretion rate
drives the visible-range photometric variation, while the NIR shows the outer
radius of the active accretion disk expands outward as the outburst progresses.
We also identify the major components of the disk system: a plane-parallel disk
atmosphere in Keplerian rotation and a 2-part warm disk wind that is collimated
near the star and wide-angle at larger radii. The wind is traced by classic
wind lines, and appears as a narrow, low-velocity, deep absorption component in
several atomic lines spanning the visible spectrum and in the CO 2.29$\mu$m
band. We compare the wind lines to those computed from wind models for other FU
Ori systems and rapidly accreting young stellar disks and find a 4000-6000 K
wind can explain the observed line profiles. Fitting the progenitor spectrum,
we find $M_* = 0.2 \ M_\odot$ and $\dot{M}_\mathrm{progenitor} = 7.8 \times
10^{-8} \ M_\odot \ \mathrm{yr}^{-1}$. Finally, we discuss HBC 722 relative to
V960 Mon, another FU Ori object we have previously studied in detail.
