  Millisecond pulsars (MSPs) have been established as a class of high-energy
($\geq$0.1 GeV) emitters with the Large Area Telescope (LAT) aboard the
\emph{Fermi Gamma-ray Space Telescope}. Most MSP gamma-ray light curves display
sharp peaks indicative of thin accelerating gaps, suggesting copious
pair-creation in the open volume. MSP gamma-ray and radio light curves have
been simulated using geometric outer-gap (OG), slot-gap/two-pole caustic (TPC),
and pair-starved polar cap gamma-ray models and either a hollow-cone beam or
altitude-limited, outer-magnetospheric gap radio model, all assuming a vacuum
retarded dipolar magnetic field geometry. A Markov chain Monte Carlo maximum
likelihood technique has been developed to find the best-fit model parameters
for nineteen MSPs using data from the LAT and various radio observatories. The
best-fit viewing angles follow a uniform, angular distribution. The
distribution of magnetic inclination angles favors all angles equally, contrary
to analyses of non-recycled pulsars, which supports the theory that MSPs have
been spun-up via accretion. There are suggestions that the radio emission
should occur nearer the light cylinder. These results have implications for MSP
population simulations and for addressing MSP contributions to diffuse
backgrounds. An implied transition in the gamma-ray luminosity versus spin-down
power trend is observed but more statistics are necessary to describe it.
