  We study the phenomenology of non-spinning eccentric binary black hole (BBH)
mergers using numerical relativity (NR) waveforms and \texttt{EccentricIMR}
waveform model, as presented in Ref. \cite{Hinder:2017sxy} (Hinder, Kidder, and
Pfeiffer, arXiv:1709.02007). This model is formulated by combining an eccentric
inspiral, derived from a post-Newtonian (PN) approximation including 3PN
conservative and 2PN reactive contributions to the BBH dynamics, with a
circular merger model. A distinctive feature of \texttt{EccentricIMR} is its
two-parameter treatment, utilizing eccentricity and mean anomaly, to
characterize eccentric waveforms. We implement the \texttt{EccentricIMR} model
in \texttt{Python} to facilitate routine use. We then validate the model
against 35 eccentric NR waveforms obtained from both the SXS and RIT NR
catalogs. We find that \texttt{EccentricIMR} model reasonably match NR data for
eccentricities up to $0.16$, specified at a dimensionless reference frequency
of $x=0.07$, and mass ratios up to $q=4$. Additionally, we use this model as a
tool for cross-comparing eccentric NR data obtained from the SXS and RIT
catalogs. Furthermore, we explore the validity of a circular merger model often
used in eccentric BBH merger modelling using both the NR data and
\texttt{EccentricIMR} model. Finally, we use this model to explore the effect
of mean anomaly in eccentric BBH mergers.
