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We computed a grid of theoretical models to fit the $\delta$ Scutifrequencies of CoRoT 100866999 detected earlier from the CoRoT timeserials. Thepulsating primary star is determined to be a main sequence star with a rotationperiod of $4.1^{+0.6}_{-0.5}$ days, rotating slower than the orbital motion.The fundamental parameters of the primary star are determined to be $M$ =$1.71^{+0.13}_{-0.04}$ $M_{\odot}$, $Z=0.012^{+0.004}_{-0.000}$, $f_{\rm ov}$ =$0.02^{+0.00}_{-0.02}$, $T_{\rm eff}$ = $8024^{+249}_{-297}$ K, $L$ =$11.898^{+2.156}_{-1.847}$ $L_{\odot}$, $\log g$ = $4.166^{+0.013}_{-0.002}$,$R$ = $1.787^{+0.040}_{-0.016}$ $R_{\odot}$, and $X_{\rm c}$ =0.488$^{+0.011}_{-0.020}$, matching well those obtained from the eclipsinglight curve analysis. Based on the model fittings, $p_1$ and $p_5$ aresuggested to be two dipole modes, and $p_3$, $p_4$, $p_6$, and $p_7$ to be fourquadrupole modes. In particular, $p_4$ and $p_7$ are identified as twocomponents of one quintuplet. Based on the best-fitting model, we find that$p_1$ is a g mode and the other nonradial modes have pronounced mixedcharacters, which give strong constraints on the convective core. Finally, therelative size of the convective core of CoRoT 100866999 is determined to$R_{\rm conv}/R$ = $0.0931^{+0.0003}_{-0.0013}$.

Exploring the convective core of the hybrid $\delta$ Scuti-$\gamma$ Doradus star CoRoT 100866999 with asteroseismology