  We present models of the H$\beta$-emitting broad-line region (BLR) in seven
Seyfert 1 galaxies from the Lick AGN (Active Galactic Nucleus) Monitoring
Project 2011 sample, drawing inferences on the BLR structure and dynamics as
well as the mass of the central supermassive black hole. We find that the BLR
is generally a thick disk, viewed close to face-on, with preferential emission
back toward the ionizing source. The dynamics in our sample range from
near-circular elliptical orbits to inflowing or outflowing trajectories. We
measure black hole masses of $\log_{10}(M_{\rm BH}/M_\odot) =
6.48^{+0.21}_{-0.18}$ for PG 1310$-$108, $7.50^{+0.25}_{-0.18}$ for Mrk 50,
$7.46^{+0.15}_{-0.21}$ for Mrk 141, $7.58^{+0.08}_{-0.08}$ for Mrk 279,
$7.11^{+0.20}_{-0.17}$ for Mrk 1511, $6.65^{+0.27}_{-0.15}$ for NGC 4593, and
$6.94^{+0.14}_{-0.14}$ for Zw 229$-$015. We use these black hole mass
measurements along with cross-correlation time lags and line widths to recover
the scale factor $f$ used in traditional reverberation mapping measurements.
Combining our results with other studies that use this modeling technique,
bringing our sample size to 16, we calculate a scale factor that can be used
for measuring black hole masses in other reverberation mapping campaigns. When
using the root-mean-square (rms) spectrum and using the line dispersion to
measure the line width, we find $\log_{10}(f_{{\rm rms},\sigma})_{\rm pred} =
0.57 \pm 0.19$. Finally, we search for correlations between $f$ and other AGN
and BLR parameters and find marginal evidence that $f$ is correlated with
$M_{\rm BH}$ and the BLR inclination angle, but no significant evidence of a
correlation with the AGN luminosity or Eddington ratio.
