We study the polarized radio emission from young Type Ia supernova remnants by means of three-dimensional numerical MHD simulations and the assumption of relativistic electron distribution related to magnetic field energy density. In our simulations, the turbulent component of background plasma is taken into account by introducing a 3D Kolmogorov-like power spectrum. The simulation results indicate (i) the different orientations of the interstellar magnetic field around SNRs and lines of sight could produce different polarized radio emission shells, (ii) the fraction of polarization may be decreased through integrating the synchrotron emissivities along the line of sight, which is mainly due to the emission from the strong turbulent and disordered region of the magnetic field, and (iii) the total intensity is strong in some regions where the polarization degree is low.