  Gaia Data Release 2 provides a wealth of data to study the internal structure
of nearby globular clusters. We use this data to investigate the internal
kinematics of 11 nearby globular clusters, with a particular focus on their
poorly-studied outer regions. We apply a strict set of selection criteria to
remove contaminating sources and create pure cluster-member samples over a
significant fraction of the radial range of each cluster. We confirm previous
measurements of rotation (or a lack thereof) in the inner regions of several
clusters, while extending the detection of rotation well beyond where it was
previously measured and finding a steady decrease in rotation with radius. We
also determine the orbital anisotropy profile and determine that clusters have
isotropic cores, are radially anisotropic out to $\approx$ 4 half-light radii
or $35\%$ of their limiting radii, and are then isotropic out to the limits of
our datasets. We detect for the first time the presence of radial anisotropy in
M 22, while confirming previous detections of radial anisotropy in 47 Tuc, M 3,
M 13, M 15, and $\omega$ Cen's innermost regions. The implications of these
measurements are that clusters can be separated into two categories: 1)
clusters with observed radial anisotropy that likely formed tidally
under-filling or are dynamically young, and 2) clusters that are primarily
isotropic that likely formed tidally filling or are dynamically old.
