  We report our analysis results for the globular cluster (GC) NGC~6341 (M92),
as a millisecond pulsar (MSP) J1717$+$4308A has recently been reported found in
this GC. The data used are from the Large Area Telescope onboard the {\it Fermi
Gamma-ray Space Telescope (Fermi)}. We detect $\gamma$-ray pulsations of the
MSP at a $4.4\sigma$ confidence level (the corresponding weighted H-test value
is $\sim$28.4). This MSP, the fourth $\gamma$-ray pulsar found in a GC, does
not have significant off-pulse emission and has $\gamma$-ray luminosity and
efficiency $1.3\times10^{34}$\,erg\,s$^{-1}$ and 1.7\% respectively. In order
to have a clear view on the properties of the known GC $\gamma$-ray MSPs, we
re-analyze the \fermi\ LAT data for the other three ones. These four MSPs share
the properties of either having high $\dot{E}$ ($\sim 10^{36}$\,erg\,s$^{-1}$)
or being in the GCs that contain only limited numbers of known MSPs. In
addition, we find that PSRs~J1823$-$3021A and B1821$-$24, in NGC~6624 and
NGC~6626 respectively, have detectable off-pulse $\gamma$-ray emission and PSR
J1835$-$3259B in NGC~6652 does not. Using the obtained off-pulse spectra or
spectral upper limits, we constrain the numbers of other MSPs in the four GCs.
The results are consistent with the numbers of the radio pulsars reported in
them. While at least in NGC~6624 and NGC~6626, the contribution of other MSPs
to their observed $\gamma$-ray emission can not be ignored, our study indicates
that the presence of a bright MSP could be the dominant factor for whether a GC
is detectable at $\gamma$-rays or not.
