  Binary black holes which are both eccentric and undergo precession remain
unexplored in numerical simulations. We present simulations of such systems
which cover about 50 orbits at comparatively high mass ratios 5 and 7. The
configurations correspond to the generic motion of a nonspinning body in a Kerr
spacetime, and are chosen to study the transition from finite mass-ratio
inspirals to point particle motion in Kerr. We develop techniques to extract
analogs of the three fundamental frequencies of Kerr geodesics, compare our
frequencies to those of Kerr, and show that the differences are consistent with
self-force corrections entering at first order in mass ratio. This analysis
also locates orbital resonances where the ratios of our frequencies take
rational values. At the considered mass ratios, the binaries pass through
resonances in one to two resonant cycles, and we find no discernible effects on
the orbital evolution. We also compute the decay of eccentricity during the
inspiral and find good agreement with the leading order post-Newtonian
prediction.
