Final averaged planet eccentricities of successfully formed resonant chains, as shown in Fig. 3. The different turbulence strengths for the individual simulations are indicated by different colors, as shown by the color bar. The dashed black line denotes the expected eccentricities of the planets (Mills et al. 2016), while the dashed red line denotes the 1σ error. For clarity, the range of eccentricities depicted on the abscissa is different for the individual plots. Unlike for the two-planet case, a dependence on turbulence strength and initial separation can be found for this case of four planets, resulting in multiple peaks in the distribution. The eccentricities of the two innermost planets do not match the measured values, while for the outer two planets, an agreement can be found. This is probably related to our implementation of the planet trap at the inner edge of the disk, which does not capture the entire physical scenario (see Sect. 4).