To investigate the mass dependence of structural transformation and star formation quenching, we construct three galaxy samples using massive (\(M_* > 10^{10} M_{\odot}\)) red, green, and blue galaxy populations at \(0.5<z<2.5\) in five 3D--{\it HST}/CANDELS fields. The structural parameters, including effective radius (\(r_{\rm e}\)), galaxy compactness (\(\Sigma_{1.5}\)), and second order moment of 20\% brightest pixels (\(M_{20}\)) are found to be correlated with stellar mass. S\'{e}rsic index (\(n\)), concentration (\(C\)), and Gini coefficient (\(G\)) seem to be insensitive to stellar mass. The morphological distinction between blue and red galaxies is found at a fixed mass bin, suggesting that quenching processes should be accompanied with transformations of galaxy structure and morphology. Except for \(r_e\) and \(\Sigma_{1.5}\) at high mass end, structural parameters of green galaxies are intermediate between red and blue galaxies in each stellar mass bin at \(z < 2\), indicating green galaxies are at a transitional phase when blue galaxies are being quenched into quiescent statuses. The similar sizes and compactness for the blue and green galaxies at high-mass end implies that these galaxies will not appear to be significantly shrunk until they are completely quenched into red QGs. For the green galaxies at \(0.5<z<1.5\), a morphological transformation sequence of bulge buildup can be seen as they are gradually shut down their star formation activities, while a faster morphological transformation is verified for the green galaxies at \(1.5<z<2.5\).