  We analyze a new numerical relativity dataset of spinning but nonprecessing
binary black holes on eccentric orbits, with eccentricities from approximately
$0.1$ to $0.5$, with dimensionless spins up to $0.75$ included at mass ratios
$q=m_1/m_2 = (1, 2)$, and further nonspinning binaries at mass ratios $q =
(1.5, 3, 4)$. A comparison of the final mass and spin of these simulations with
noneccentric data extends previous results in the literature on circularization
of eccentric binaries to the spinning case. For the $(l,m)=(2,2)$ spin-weighted
spherical harmonic mode we construct eccentric hybrid waveforms that connect
the numerical relativity data to a post-Newtonian description for the inspiral,
and we discuss the limitations in the current knowledge about post-Newtonian
theory which complicate the generation of eccentric hybrid waveforms. We also
perform a Bayesian parameter estimation study, quantifying the parameter biases
introduced when using three different quasicircular waveform models to estimate
the parameters of highly eccentric binary systems. We find that the used
aligned-spin quasicircular model including higher order modes produces lower
bias in certain parameters than the nonprecessing quasicircular model without
higher order modes and the quasicircular precessing model.
