Fast Radio Bursts (FRBs) are extra-galactic origin milli-second duration bright radio bursts. Theoretically, FRBs may produce optical counterparts with durations from milliseconds to hours. The FRB optical counterparts may be detectable in future large field telescopes in China, including the China Space Station Survey Space Telescope (CSST), the 2.5-meter Large Field Survey Telescope (WFST) of the University of Science and Technology of China (USTC), and the Purple Mountain Observatory (PMO), and Earth 2.0 (ET). The fast radio burst optical counterparts are grouped into millisecond time-scale optical counterparts, hourly time-scale optical counterparts, and optical afterglow for our study. The first two can be generated by the high-energy extension of FRBs or the radio radiation of fast radio bursts and the inverse Compton scattering of high-energy electrons. The event rates highly depend on the optical-radio flux ratio $\eta_\nu$. For millisecond duration optical counterparts, the detection rate of WFST, CSST,and ET can reach hundreds per year in an ideal case. If $\eta_\nu$~ 10^-3, the corresponding annual detectionrates of WFST and CSST are in the order of 1, and the annual detection rate of ET is 19.5. For the hourly optical counterparts, ideally, the age of the supernova remnant is 5 years, $\eta_\nu$ is about 10^-6, and the annual detection rates are above 100. The X-ray counterpart of FRB 200428 indicates that FRBs may produce relativistic out ow, which will interact with the interstellar medium to produce optical afterglows. Combined with the standard afterglow model, the detectability of optical afterglow is explored with a simulation of fast radio bursts following the redshift and energy distribution from the literature.With a total energy-radio energy ratio similar to FRB 200428, ζ = 105, the estimated annual detection rates of CSST, WFST, and ET are 1.3, 1.0, and 67, respectively.