  We analyze more than 15 years of the \gr\ data, obtained with the Large Area
Telescope (LAT) onboard {\it the Fermi Gamma-ray Space Telescope (Fermi)}, for
the region of the young supernova remnant (SNR) RCW~103, since the nearby
source 4FGL J1616.2$-$5054e, counterpart to HESS~J1616$-$518 and
$\simeq$13\,arcmin away from the SNR, is determined to be extended in the more
recent Fermi-LAT source catalog. Different templates for 4FGL J1616.2$-$5054e
and RCW~103 are tested, and we find that a point source with a power-law (PL)
spectrum at the southern limb of the SNR best describes the detected gamma-ray
emission. The photon index of the PL emission is $\Gamma\simeq 2.31$(or
$\alpha\simeq 2.4$ in a Log-Parabola model) , softer than the previously
reported $\Gamma\simeq 2.0$ when the counterpart to HESS~J1616$-$518 was
considered to be a point source (which likely caused mis-identification of
extended emission at RCW~103). In order to produce the \gr\ emission in a
hadronic scenario, we estimate that protons with an index$\sim$2.4 PL energy
distribution are needed. These results fit with those from multi-wavelength
observations that have indicated the remnant at the southern limb is
interacting with a molecular cloud.
