Same as Figure 4, but as a function of the initial inclination dispersion of protoplanets (﹩\langle {i}_{\mathrm{ini}}^{2}{\rangle }^{1/2}﹩). The cross symbols are the results of model N32. The initial eccentricity dispersions are ﹩\langle {e}_{\mathrm{ini}}^{2}{\rangle }^{1/2}={10}^{-1.5}﹩ rad (red circles), and ﹩\langle {e}_{\mathrm{ini}}^{2}{\rangle }^{1/2}={10}^{-3}﹩ rad (blue triangles). The dotted lines are the best-fit eccentricity (e = 0.049) and the mode of the mutual inclination (0.017 rad < i < 0.039 rad) of the Kepler planets (Fabrycky et al. 2014; Hadden & Lithwick 2014; Van Eylen & Albrecht 2015). The solid and dashed lines are the fits by the least-squares-fit method for models N16 and N8 using Equation (4). The coefficients are summarized in Table 3.