  In the first three observation runs, ground-based gravitational wave (GW)
detectors have observed close to 100 compact binary coalescence (CBC) events.
The GW detection rates for CBCs are expected to increase with improvements in
the sensitivity of the International Gravitational-Wave Observatory Network
(IGWN). However, with improved sensitivity, non-Gaussian instrumental
transients or ``glitches'' are expected to adversely affect GW searches and
characterisation algorithms. The most detrimental effect is due to
short-duration glitches, which mimic the morphology of short-duration GW
transients, in particular Intermediate-mass black hole (IMBH) binaries. They
can be easily misidentified as astrophysical signals by current searches, and
if included in astrophysical analyses, glitches mislabelled as IMBH binaries
can affect IMBH population studies. In this work, we introduce a new similarity
metric that quantifies the consistency of astrophysical parameters across the
detector network and helps to distinguish between IMBH binaries and
short-duration, loud glitches which mimic such binaries. We develop this method
using a simulated set of IMBH binary signals and a collection of noise
transients identified during the third observing run of the Advanced LIGO and
Advanced Virgo detectors.
