  I review our understanding of the structure and kinematics of the Large
Magellanic Cloud (LMC), with a particular focus on recent results. This is an
important topic, given the status of the LMC as a benchmark for studies of
microlensing, tidal interactions, stellar populations, and the extragalactic
distance scale. I address the observed morphology and kinematics of the LMC;
the angles under which we view the LMC disk; its in-plane and vertical
structure; the LMC self-lensing contribution to the total microlensing optical
depth; the LMC orbit around the Milky Way; and the origin and interpretation of
the Magellanic Stream. Our understanding of these topics is evolving rapidly,
in particular due to the many large photometric and kinematic datasets that
have become available in the last few years. It has now been established that:
the LMC is considerably elongated in its disk plane; the LMC disk is thicker
than previously believed; the LMC disk may have warps and twists; the LMC may
have a pressure-supported halo; the inner regions of the LMC show unexpected
complexities in their vertical structure; and precession and nutation of the
LMC disk plane contribute measurably to the observed line-of-sight velocity
field. However, many open questions remain and more work is needed before we
can expect to converge on a fully coherent structural, dynamical and
evolutionary picture that explains all observed features of the LMC.
