  Theoretical models suggest that intermediate mass black holes (IMBHs) may
form and reside in the centers of globular clusters. IMBHs are still elusive to
observations, but the accelerations of pulsars may bring along a unique
fingerprint of their presence. In this work, we focus on the pulsars in the
globular cluster M62. Using the new distance of M62 obtained from Gaia
observations, we find that the measured pulsars' accelerations suggest a
central excess of mass in the range [1200, 6000]$M_{\odot}$, corresponding to
[0.2, 1] percent of the current total mass of the cluster. Our analysis can not
unambiguously discriminate between an IMBH or a system of stellar mass dark
remnants of comparable total mass.
