Notes. Column #1: ID of the knots reported in Fig. 2; #2: delensed magnitudes at 1600 Å; #3: Adopted E(B − V): 0.15 for knot 5.1 as derived by Chisholm et al. (2019), and the mean value inferred from the SED fitting for the other knots (see text for details); #4: Assumed ages in Myr. The age of 3 Myr has been adopted for 5.1 (Chisholm et al. 2019), and ages ≳7 Myr is assumed for the others. #5: delensed effective radii at 1600 Å as derived from Galfit modeling. Only 5.1 is resolved, whereas the radii of the other knots are upper limits; #6: stellar mass in units of ×10⁶ M_⊙ derived at the age reported in Col. #3, accordingly to the adopted instantaneous burst of Starburst99 models, Z = 0.008 Z_⊙ and Salpeter IMF with M_UP = 100 M_⊙. Being the ages lower limits, also the stellar masses are formally lower limits; #7: total magnification from the best solution of the lens model (see Sect. 3.1); #8: tangential magnification from the best solution of the lens model (see Sect. 3.1); #9: dynamical age adopting the ages (#4), stellar mass (#6) and size (#5) (see text for details). The limits on sizes and stellar masses imply such values tend to be lower limits; #10: age and stellar mass at Π = 1, given with the same units as Cols. #4 and #6, respectively; (†) Host galaxy parameters as derived from the SED-fitting procedure described in Sect. 4.1; see also Fig. 4 where the 68% central confidence interval is reported; (*) individual knots used in this manuscript to infer the cluster formation efficiency. Results from the multiple images of knot 5.1(1,b,c,h,i,l,m,n) are shown in the top part of the table. Knots 5.7c,d and 5.10 are multiple images of a possible stellar transient object describe by Vanzella et al. (2020c) and are not included here. The knot 5.14 is also not included in this work since it is currently tentatively associated with multiple images of the knot 5.4.