**Table 3:** Fate of the disk mass at the end of each run: results for scenarios without ( $\nrightarrow$ ) and with ( $\rightarrow$ ) type I migration.
Scenario	I $\nrightarrow$	I $\rightarrow$	IV $\nrightarrow$	IV $\rightarrow$	V $\nrightarrow$	V $\rightarrow$
Total initial solids $({M}_{\oplus})$	24.81	24.81	24.81	24.81	24.81	23.47
Total surviving solids $({M}_{\oplus})$	16.60 (67%)	18.70 (75%)	21.23 (86%)	15.13 (61%)	20.22 (81%)	18.23 (78%)
Interior surviving solids $({M}_{\oplus})$	0.88 (4%)	3.44 (14%)	0.84 (3%)	1.84 (7%)	0.31 (1%)	6.23 (27%)
$N, f_{{\rm proto}}$	0, 0	1, 0.99	0, 0	1, 0.96	0, 0	1, 1
Exterior surviving solids $({M}_{\oplus})$	15.72 (63%)	15.27 (62%)	20.39 (82%)	13.29 (54%)	19.90 (80%)	12.00 (51%)
$N, f_{{\rm proto}}$	39, 0.27	34, 0.22	31, 0.63	9, 0.34	23, 0.66	7, 0.24
Accreted by star $({M}_{\oplus})$	0.01 (0.04%)	0.0 (0%)	0.0 (0%)	0.0 (0%)	0.0 (0%)	0.01 (0.04%)
Accreted by giant $({M}_{\oplus})$	8.20 (33%)	6.01 (24%)	3.41 (14%)	9.68 (39%)	4.59 (19%)	5.23 (22%)
Ejected $({M}_{\oplus})$	0.00 (0%)	0.1 (0.4%)	0.17 (1%)	0.0 (0%)	0.0 (0%)	0.0 (0%)

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