  There are two classes of gamma-ray transients with a duration shorter than 2
seconds. One consists of cosmic short Gamma-Ray Bursts (GRBs) taking place in
the deep universe via the neutron star mergers, and the other is the magnetar
giant flares (GFs) with energies of $\sim 10^{44}-10^{46}$ erg from ``nearby"
galaxies. Though the magnetar GFs and the short GRBs have rather similar
temporal and spectral properties, their energies ($E_{\rm \gamma,iso}$) are
different by quite a few orders of magnitude and hence can be distinguished
supposing the host galaxies have been robustly identified. The newly observed
GRB 231115A has been widely discussed as a new GF event for its high
probability of being associated with M82. Here we conduct a detailed analysis
of its prompt emission observed by Fermi-GBM, and compare the parameters with
existing observations. The prompt gamma-ray radiation properties of GRB
231115A, if associated with M82, nicely follow the $E_{\rm p,z}-E_{\gamma,\rm
iso}$ relation of the GFs, where $E_{\rm p,z}$ is the peak energy of the
gamma-ray spectrum after the redshift ($z$) correction. To be a short GRB, the
reshift needs to be $\sim 1$. Though such a chance is low, the available
X-ray/GeV observation upper limits are not stringent enough to further rule out
this possibility. We have also discussed the prospect of convincingly
establishing the magnetar origin of GRB 231115A-like events in the future.
