  We present new radial velocity measurements from the Magellan and the
Anglo-Australian Telescopes for 174 previously known and 122 newly confirmed
globular clusters (GCs) around NGC 5128, the nearest accessible massive
early-type galaxy at D=3.8 Mpc. Remarkably, 28 of these newly confirmed GCs are
at projected radii >50' ($\gtrsim 54$ kpc), extending to $\sim 130$ kpc, in the
outer halo where few GCs had been confirmed in previous work. We identify
several subsets of GCs that spatially trace halo substructures that are visible
in red giant branch star maps of the galaxy. In some cases, these subsets of
GCs are kinematically cold, and may be directly associated with and originate
from these specific stellar substructures. From a combined kinematic sample of
645 GCs, we see evidence for coherent rotation at all radii, with a higher
rotation amplitude for the metal-rich GC subpopulation. Using the tracer mass
estimator, we measure a total enclosed mass of $2.5\pm0.3 \times 10^{12}
M_{\odot}$ within $\sim 120$ kpc, an estimate that will be sharpened with
forthcoming dynamical modeling. The combined power of stellar mapping and GC
kinematics makes NGC 5128 an ongoing keystone for understanding galaxy assembly
at mass scales inaccessible in the Local Group.
