  We used two numerical models, namely the \texttt{CBwaves} and
\texttt{SEOBNRE} algorithms, based on the post-Newtonian and effective-one-body
approaches for binary black holes evolving on eccentric orbits. We performed
20.000 new simulations for non-spinning and 240.000 simulations for
aligned-spin configurations on a common grid of parameter values over the
parameter space spanned by the mass ratio $q\equiv m_1/m_2\in[0.1,\,1]$, the
gravitational mass $m_i \in [10M_\odot,\, 100M_\odot]$ of each component
labeled by $i$, the corresponding spin magnitude $S_i \in [0,\,0.6]$ and a
constant initial orbital eccentricity $e_{0}$. A detailed investigation was
conducted to ascertain whether there was a discrepancy in the waveforms
generated by the two codes. This involved an in-depth analysis of the mismatch.
Furthermore, an extensive comparison was carried out on the outlier points
between the two codes.
