  The star cluster (SC) age distribution of the Large Magellanic Cloud (LMC)
exhibits a gap from $\sim$ 4 to 10 Gyr ago, with an almost total absence of
SCs. Within this age gap, only two confirmed SCs have been identified hitherto.
Nonetheless, the star field counterpart does not show the same characteristics,
making the LMC a peculiar galaxy where star formation history and cluster
formation history appear to differ significantly. We re-analyzed the
color-magnitude diagram (CMD) of the KMHK 1762 SC by using the deep optical
photometry provided by the "Yes, Magellanic Clouds Again" survey, to robustly
assess its age. First, we partially removed foreground and/or field stars by
means of parallaxes and proper motions obtained from the {\it Gaia} Early Data
Release 3. Then, we applied the Automated Stellar Cluster Analysis package to
the cleaned photometric catalogue to identify the isochrone that best matches
the CMD of KMHK 1762. The estimated age of KMHK 1762 is $\log (t) = 9.74 \pm
0.15$ dex ($\sim$5.5 Gyr), that is more than 2 Gyr older than the previous
estimation which was obtained with shallower photometry. This value makes KMHK
1762 the third confirmed age gap SC of the LMC. The physical existence of a
quiescent period of the LMC SC formation is questioned. We suggest it can be
the result of an observational bias, originated by the combination of shallow
photometry and limited investigation of the LMC periphery.
