  Based on the two-minutes TESS data, we analyzed intrinsic oscillations of the
primary component and identified seven confident independent $\delta$ Scuti
frequencies ($f_1$, $f_2$, $f_3$, $f_4$, $f_7$, $f_{11}$, and $f_{12}$). Both
of single-star evolutionary models and mass-accreting models are computed to
reproduce the $\delta$ Scuti freqiencies. Fitting results of them match well
with each other. The stellar parameters of the primary star yielded by
asteroseismology are $M$ = $1.92^{+0.10}_{-0.02}$ $M_{\odot}$, $Z$ =
0.011$^{+0.006}_{-0.001}$, $R$ = $2.068^{+0.050}_{-0.007}$ $R_{\odot}$, $\log
g$ = $4.090^{+0.010}_{-0.002}$, $T_{\rm eff}$ = $8346^{+244}_{-320}$ K, $L$ =
$18.65^{+3.31}_{-2.82}$ $L_{\odot}$, which match well with the dynamic ones by
the binary model. Furthermore, our asteroseismic results show that OO Dra is
another Algol system that has just undergone the rapid mass-transfer stage.
Fitting results of single-star evlutionary models indicate that the pulsator is
helium-poor star with an age of 8.22$^{+0.12}_{-1.33}$ Myr, and the further
mass-accreting models show that the primary star looks like an almost unevolved
star formed by an extremely helium-poor mass accretion in Case A evolutionary
scenario.
