  Eclipsing binary systems are significant objects for astrophysics in that
direct observations can determine the fundamental parameters of stars. In this
study, we determined precisely the fundamental parameters of the binary
component stars obtained by simultaneous analysis of radial velocities and the
{\it TESS} light curve using the Wilson and Devinney code. Following the
analysis, the masses and radii of the primary and secondary components were
determined as $M_{1}= 1.58\pm 0.01M_\odot$, $M_{2}= 0.48\pm0.02M_\odot$, and
$R_{1}=1.93\pm 0.01R_\odot$, $R_{2}= 1.14\pm 0.01 R_\odot$, respectively.
Furthermore, the distance of IS CMa is calculated as $92.7\pm6.5$ pc. On the
basis of the analysis of the mid-eclipse times, it was found that the variation
in the orbital period is represented by an upward parabola. It has an
increasing rate of $dP/dt$ = 1.09 $\times$ 10$^{-7}$ day yr$^{-1}$. Using
PARSEC stellar evolutionary tracks and isochrones with solar metallicity were
estimated the age of IS CMa as $1.3\pm0.1$ Gyr. Kinematic and Galactic orbital
parameters of IS CMa were obtained from the astrometric and spectroscopic data
of the system. The Galactic orbit analysis reveals that IS CMa formed inside
the solar circle and it is a member of the young thin-disc population.
