  We compare the properties of gas flows on both the near and far side of the
Large Magellanic Cloud (LMC) disk using Hubble Space Telescope UV
absorption-line observations toward an AGN behind (transverse) and a star
within (down-the-barrel) the LMC disk at an impact parameter of 3.2 kpc. We
find that even in this relatively quiescent region gas flows away from the disk
at speeds up to $\sim$100 km/s in broad and symmetrical absorption in the low
and high ions. The symmetric absorption profiles combined with previous surveys
showing little evidence that the ejected gas returns to the LMC and provide
compelling evidence that the LMC drives a global, large-scale outflow across
its disk, which is the likely result of a recent burst of star formation in the
LMC. We find that the outflowing gas is multiphase, ionized by both
photoionization (SiII and SiIII) and collisional ionization (SiIV and CIV). We
estimate a total mass and outflow rate to be $>10^7$ Msun and $>0.4$ Msun/yr.
Since the velocity of this large-scale outflow does not reach the LMC escape
velocity, the gas removal is likely aided by either ram-pressure stripping with
the Milky Way halo or tidal interactions with the surrounding galaxies,
implying that the environment of LMC-like or dwarf galaxies plays an important
role in their ultimate gas starvation. Finally we reassess the mass and
plausible origins of the high-velocity complex toward the LMC given its
newly-determined distance that places it in the lower Milky Way halo and
sky-coverage that shows it extends well beyond the LMC disk.
