  Using archival {\it Fermi}-LAT data with a time span of $\sim12$ years, we
study the population of Millisecond Pulsars (MSPs) in Globular Clusters (GlCs)
and investigate their dependence on cluster dynamical evolution in the Milky
Way Galaxy. We show that the $\gamma$-ray luminosity ($L_{\gamma}$) and
emissivity ($\epsilon_{\gamma}=L_{\gamma}/M$) are good indicators of the
population and abundance of MSPs in GlCs, and they are highly dependent on the
dynamical evolution history of the host clusters. Specifically speaking, the
dynamically older GlCs with more compact structures are more likely to have
larger $L_{\gamma}$ and $\epsilon_{\gamma}$, and these trends can be summarized
as strong correlations with cluster stellar encounter rate $\Gamma$ and the
specific encounter rate ($\Lambda=\Gamma/M$), with $L_{\gamma}\propto
\Gamma^{0.70\pm0.11}$ and $\epsilon_{\gamma}\propto \Lambda^{0.73\pm0.13}$ for
dynamically normal GlCs. However, as GlCs evolve into deep core collapse, these
trends are found to be reversed, implying that strong encounters may have lead
to the ejection of MSPs from core-collapsed Systems. Besides, the GlCs are
found to exhibit larger $\epsilon_{\gamma}$ with increasing stellar mass
function slope, decreasing tidal radius and distances from the Galactic Center
(GC). These correlations indicate that, as GlCs losing kinetic energy and
spiral in towards GC, tidal stripping and mass segregation have a preference in
leading to the loss of normal stars from GlCs, while MSPs are more likely to
concentrate to cluster center and be deposited into the GC. Moreover, we gauge
$\epsilon_{\gamma}$ of GlCs is $\sim10-1000$ times larger than the Galactic
bulge, the latter is thought to reside thousands of unresolved MSPs and may
responsible for the GC $\gamma$-ray excess, which support that GlCs are
generous contributors to the population of MSPs in the GC.
