  Four-color charge-coupled device (CCD) light curves in $B$, $V$, $Rc$ and
$Ic$ bands of the total-eclipsing binary system, V1853 Ori, are presented. By
comparing our light curves with those published by previous investigators, it
is detected that the O'Connell effect on the light curves is disappeared. By
analyzing those multi-color light curves with the Wilson-Devinney code (W-D
code), it is discovered that V1853 Ori is an A-type intermediate-contact binary
with a degree of contact factor of $f=33.3\%(3.7\%)$ and a mass ratio of
$q=0.1896(0.0013)$. Combining our 10 new determined times of light minima
together with the others published in the literature, the period changes of the
system is investigated. We found that the general trend of the
observed-calculated $(O-C)$ curve shows a downward parabolic variation that
corresponds to a long-term decrease in the orbital period with a rate of
$dP/dt=-1.96(0.46)\times{10^{-7}}$ d yr$^{-1}$. The long-term period decrease
could be explained by mass transfer from the more-massive component to the
less-massive one. By combining our photometric solutions with the Gaia DR 2
data, absolute parameters were derived as $M_{1}$ = 1.20 M$_{\odot}$, $M_{2}$ =
0.23 M$_{\odot}$, $R_{1}$ = 1.36 R$_{\odot}$, and $R_{2}$ = 0.66 R$_{\odot}$.
The long-term period decrease and the intermediate-contact configuration
suggest that V1853 Ori will evolve into a high fill-out overcontact binary.
