  We present detailed analyses of updated eclipse timing diagrams for 32
contact binary merger candidates in the Galactic bulge. The photometric data
was obtained from 2016 to 2021 using the Korea Microlensing Telescope Network
(KMTNet) with the 1.6 m telescopes located at three southern sites (CTIO, SAAO,
and SSO). The times of minimum lights were determined by applying the binary
star model to full light curves created at half-year intervals from the
observations. The orbital period variations of the binary systems were analyzed
using the $O-C$ diagrams from our new timings with the others published in the
literature (Hong et al.), which are based on the OGLE observations from 2001 to
2015. As results, the orbital periods and period decreasing rates of 32 binary
systems were located to be in the ranges of 0.370$-$1.238 days and from $-3.0$
to $-13.1\times10^{-6}$ day yr$^{-1}$, respectively. Out of these stars, 24
systems show a combination effect of a parabola and a light travel time caused
by a third body and their outer orbital periods are in the range of 9.1$-$26.5
yr, respectively. We propose that all of our merger candidates need additional
monitoring observations to study a luminous red nova (LRN) progenitor.
