  There is growing evidence from stellar kinematics and galactic chemical
evolution (GCE) suggesting that giant planets (M$_{P}\geq$0.3$M_{J}$) are
relatively young compared to the most commonly occurring population of small
planets (M$_{P} <$0.3$M_{J}$). To further test the validity of these results,
we analyzed the ages for a large number of 2336 exoplanet hosting stars
determined using three different but well-established isochrone fitting models,
namely, PARSEC, MIST, and Yonsei Yale (YY). As input parameters, we used Gaia
DR3 parallaxes, magnitudes, and photometric temperature, as well as
spectroscopically determined more accurate temperatures and metallicities from
the Sweet Catalog. Our analysis suggests that $\sim$~50$\%$ to 70$\%$ of stars
with planets are younger than the sun. We also find that, among the confirmed
exoplanetary systems, stars hosting giant planets are even younger compared to
small planet hosts. The median age of $\sim$~2.61 to 3.48~Gyr estimated for the
giant planet-hosting stars (depending on the model input parameters) suggests
that the later chemical enrichment of the galaxy by the iron-peak elements,
largely produced from Type Ia supernovae, may have paved the way for the
formation of gas giants. Furthermore, within the giant planet population
itself, stars hosting hot Jupiters (orbital period $\le$10 days) are found to
be younger compared to the stellar hosts of cool and warm Jupiters (orbital
period $>$10 days), implying that hot Jupiters could be the youngest systems to
emerge in the progression of planet formation.
