  In this paper, we continue our study of the motion of spinning test bodies
orbiting Kerr black holes. Non-spinning test bodies follow geodesics of the
spacetime in which they move. A test body's spin couples to the curvature of
that spacetime, introducing a "spin-curvature force" which pushes the body's
worldline away from a geodesic trajectory. The spin-curvature force is an
important example of a post-geodesic effect which must be modeled carefully in
order to accurately characterize the motion of bodies orbiting black holes. One
motivation for this work is to understand how to include such effects in models
of gravitational waves produced from the inspiral of stellar mass bodies into
massive black holes. In this paper's predecessor, we describe a technique for
computing bound orbits of spinning bodies around black holes with a
frequency-domain description which can be solved very precisely. In that paper,
we present an overview of our methods, as well as present results for orbits
which are eccentric and nearly equatorial (i.e., the orbit's motion is no more
than $\mathcal{O}(S)$ out of the equatorial plane). In this paper, we apply
this formulation to the fully generic case -- orbits which are inclined and
eccentric, with the small body's spin arbitrarily oriented. We compute the
trajectories which such orbits follow, and compute how the small body's spin
affects important quantities such as the observable orbital frequencies
$\Omega_r$, $\Omega_\theta$ and $\Omega_\phi$.
