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We present new spectroscopic observations of the double-lined eclipsingbinary V2653\,Oph. The photometric observations obtained by $ASAS$ wereanalysed and combined with the analysis of radial velocities for deriving theabsolute parameters of the components. Masses and radii were determined for thefirst time as M$_p$=1.537$\pm$0.021 M$_{\odot}$ and R$_p$=2.215$\pm$0.055R$_{\odot}$, M$_s$=1.273$\pm$0.019 M$_{\odot}$ and R$_s$=2.000$\pm$0.056R$_{\odot}$ for the components of V2653\,Oph. We estimate an interstellarreddening of 0.15$\pm$0.08\,mag and a distance of 300$\pm$50\,pc for thesystem, both supporting the membership of the open cluster Collinder\,359.Using the out-of-eclipse photometric data we have made frequency analysis anddetected a periodic signal at 1.0029$\pm$0.0019\,c/d. This frequency and thelocation of the more massive star on the HR diagram lead to classification of a$\gamma$ Dor type variable. Up to date only eleven $\gamma$ Dor type pulsatorsin the eclipsing binaries have been discovered. For six out of 11 systems, thephysical parameters were determined. Although a small sample, we find empiricalrelations that $P_{puls}$ $\propto$ $P_{orb}^{0.43}$ and $P_{puls}$ $\propto$$g^{-0.83}$. While the pulsation periods increase with longer orbital periods,they decrease with increasing surface gravities of pulsating components andgravitational pull exerted by the companions. We present, briefly, theunderlying physics behind

V2653 Ophiuchii with a pulsating component and Ppuls-Porb, Ppuls-g correlations for gamma-Dor type pulsators