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} $.