In this paper , we investigate the formation of terrestrial planets in the late stage of planetary formation using two-planet model .
At that time , the protostar has formed for about 3 Myr and the gas disk has dissipated .
In the model , the perturbations from Jupiter and Saturn are considered .
We also consider variations of the mass of outer planet , and the initial eccentricities and inclinations of embryos and planetesimals .
Our results show that , terrestrial planets are formed in 50 Myr , and the accretion rate is about 60 \% - 80 \% .
In each simulation , 3 - 4 terrestrial planets are formed inside ” Jupiter ” with masses of 0.15 - 3.6 M _ { \oplus } .
In the 0.5 - 4 AU , when the eccentricities of planetesimals are excited , planetesimals are able to accrete material from wide radial direction .
The plenty of water material of the terrestrial planet in the Habitable Zone may be transferred from the farther places by this mechanism .
Accretion could also happen a few times between two major planets only if the outer planet has a moderate mass and the small terrestrial planet could survive at some resonances over time scale of 10 ^ { 8 } yr .
In one of our simulations , com-mensurability of the orbital periods of planets is very common .
Moreover , a librating-circulating 3:2 configuration of mean motion resonance is found .