  Recently K2 and TESS have discovered transiting planets with radii between
$\sim$ 5-10 R$_\oplus$ around stars with ages $<100$ Myr. These young planets
are likely to be the progenitors of the ubiquitous super-earths/sub-neptunes,
that are well studied around stars with ages $\gtrsim 1$ Gyr. The formation and
early evolution of super-earths/sub-neptunes are poorly understood. Various
planetary origin scenarios predict a wide range of possible formation
entropies. We show how the formation entropies of young ($\sim$20-60 Myr),
highly irradiated planets can be constrained if their mass, radius and age are
measured. This method works by determining how low-mass a H/He envelope a
planet can retain against mass-loss. This lower bound on the H/He envelope mass
can then be converted into an upper bound on the entropy. If planet mass
measurements with errors $\lesssim 20$\% can be achieved for the discovered
young planets around DS Tuc A and V1298 Tau, then insights into their origins
can be obtained. For these planets, higher measured planet masses would be
consistent with standard core-accretion theory. In contrast, lower planet
masses ($\lesssim 6-7$ M$_\oplus$) would require a "boil-off" phase during
protoplanetary disc dispersal to explain.
