  We perform spatial and spectral analyses of the Large Magellanic Cloud (LMC)
gamma-ray emission collected over 66 months by the Fermi Gamma-ray Space
Telescope. In our spatial analysis, we model the LMC cosmic-ray distribution
and gamma-ray production using observed maps of the LMC interstellar medium,
star formation history, interstellar radiation field, and synchrotron emission.
We use bootstrapping of the data to quantify the robustness of spatial model
performance. We model the LMC gamma-ray spectrum using fitting functions
derived from the physics of $\pi^0$ decay, bremsstrahlung, and inverse Compton
scattering. We find the integrated gamma-ray flux of the LMC from 200 MeV to 20
GeV to be $1.38 \pm 0.02 \times 10^{-7}$ ph cm$^{-2}$ s$^{-1}$, of which we
attribute about 10% to inverse Compton scattering and 40% to bremsstrahlung.
From our work, we conclude that the spectral index of the LMC cosmic-ray proton
population is 2.4$\pm$0.2, and we find that cosmic-ray energy loss through
gamma-ray production is concentrated within a few hundred pc of acceleration
sites. Assuming cosmic-ray energy equipartition with magnetic fields, we
estimate LMC cosmic rays encounter an average magnetic field strength ~3
$\mu$G.
