  We present a Parkes multibeam \HI survey of the Large Magellanic Cloud (LMC).
This survey, which is sensitive to spatial structure in the range 200 pc to 10
kpc, complements the Australia Telescope Compact survey, which is sensitive to
structure in the range 15 pc to 500 pc. With an rms column density sensitivity
of 8 x 10^16/cm^2 for narrow lines and 4 x 10^17/cm^2 for typical linewidths of
40 km/s, emission is found to be extensive well beyond the main body of the
LMC. Arm-like features extend from the LMC to join the Magellanic Bridge and
the Leading Arm, a forward counterpart to the Magellanic Stream. These
features, whilst not as dramatic as those in the SMC, appear to have a common
origin in the Galactic tidal field, in agreement with recent 2MASS and DENIS
results for the stellar population. The diffuse gas which surrounds the LMC,
particularly at pa's 90 to 330 deg, appears to be loosely associated with tidal
features, but loosening by the ram pressure of tenuous Galactic halo gas
against the outer parts of the LMC cannot be discounted. High-velocity clouds,
which lie between the Galaxy and the LMC in velocity and which appear in the UV
spectra of some LMC stars, are found to be associated with the LMC if their
heliocentric velocity exceeds about +100 km/s. They are possibly the product of
energetic outflows from the LMC disk. The HI mass of the LMC is found to be
(4.8+/-0.2) x 10^8 Msun (for an assumed distance of 50 kpc), substantially more
than previous recent measurements.
