  We present CIV BLR modeling results for the multiply imaged $z=2.805$ quasar
SDSS J2222+2745. Using data covering a 5.3 year baseline after accounting for
gravitational time delays, we find models that can reproduce the observed
emission-line spectra and integrated CIV fluctuations. The models suggest a
thick disk BLR that is inclined by $\sim$40 degrees to the observer's line of
sight and with a emissivity weighted median radius of $r_{\rm median} =
33.0^{+2.4}_{-2.1}$ light days. The kinematics are dominated by near-circular
Keplerian motion with the remainder inflowing. The rest-frame lag one would
measure from the models is $\tau_{\rm median} = 36.4^{+1.8}_{-1.8}$ days, which
is consistent with measurements based on cross-correlation. We show a possible
geometry and transfer function based on the model fits and find that the
model-produced velocity-resolved lags are consistent with those from
cross-correlation. We measure a black hole mass of $\log_{10}(M_{\rm
BH}/M_\odot) = 8.31^{+0.07}_{-0.06}$, which requires a scale factor of
$\log_{10}(f_{{\rm mean},\sigma}) = 0.20^{+0.09}_{-0.07}$.
