  Millisecond pulsars can serve as effective probes to investigate the presence
of Intermediate-mass Black Holes (IMBHs) within Galactic globular clusters
(GCs). Based on the standard structure models for GCs, we conduct simulations
to analyze the distributions of pulsar accelerations within the central region
of NGC 6517. By comparing the measured accelerations of pulsars obtained from
their period derivatives $\dot P$ to the simulated distribution profiles, we
demonstrate that a central excess of dark mass is required to account for the
measured accelerations. Our analysis, which relies on existing pulsar timing
observations, is currently unable to differentiate between two possible
scenarios: an IMBH precisely situated at the core of the cluster with mass
$\gtrsim 9000^{+4000}_{-3000}~M_{\odot}$, or a central concentration of stellar
mass dark remnants with a comparable total mass. However, with additional
acceleration measurements from a few more pulsars in the cluster, it will be
possible to differentiate the source of the nonluminous matter.
