  Gravitational wave detections offer insights into the astrophysical
populations of black holes in the universe and their formation processes.
Detections of binaries consisting of black holes lying outside the bulk
distribution of the astrophysical population are particularly intriguing. In
this study, we perform an injection analysis within the intermediate-mass black
hole range, utilizing the NR surrogate model NRSur7dq4 and a selection of NR
waveforms from the SXS and RIT catalogues. Our investigation focuses on the
detectability of precession and its potential degeneracy with eccentricity,
especially for short signals with only a few cycles in band. While total mass,
mass ratio, and $\chi_\mathrm{eff}$ are generally well recovered, the recovery
of $\chi_\mathrm{p}$ is largely limited, and noise significantly impacts the
recovery of some parameters for short signals. We also find that eccentricity
lower than 0.2 is insufficient to mimic precession in parameter estimation when
assuming a quasi-circular signal. Our results suggest that a certain degree of
precession is necessary to produce evidence of high precession in parameter
estimation, but it remains challenging to conclusively determine which effect
is responsible for the high precession observed in events like GW190521. We
emphasize the importance of caution when interpreting properties of a binary
from short signals and highlight the potential benefits of future third
generation detectors and eccentric waveform models for more exhaustive
exploration of parameter space.
