our target area. Figure \[fig1\]c shows the boundary of each NVSS clump against the locations of earlier reported O4-7(super)-giant stars (see filled stars). A broken box is indicated in Figures \[fig1\]a, \[fig1\]b and \[fig1\]c, which shows the area investigated by @kohno18. The ionized clumps (see IDs \#c10, \#c8, and \#c1–c7) are found toward the MIR bubbles [i.e., N10 and N11; @churchwell06; @gama16], G013.210$-$0.144 [@white05], and the W33 complex (W33 A (G012.90$-$0.24, G012.90$-$0.26), W33 B (G012.68$-$0.18), and W33 Main (G012.81$-$0.19); see Figure \[fig1\]c), where we also find extended warm dust emission at 24 $\mu$m (see Figure \[fig1\]b). Two massive O4-7(super)-giant stars (i.e., \#7 and \#8) are seen toward the NVSS clump \#c3, while a massive O4-7(super)-giant star \#23 is found in the direction of the NVSS clump \#c4 (see Figure \[fig1\]c).

Following the work of @dewangan17, we have estimated the number of Lyman continuum photons [$N_\mathrm{uv}$; see @panagia73; @matsakis76] and the dynamical age [$t_\mathrm{dyn}$; see @dyson80] of each ionized clump (see Table \[tab2\]). Previously, @kohno18 adopted an initial particle number density of the ambient neutral gas (i.e., $n_{0}$ = 10$^{4}$ cm$^{-3}$) in the estimations of the formation timescale of the H[ii]{} regions G012.745$-$00.153 and G012.820$-$00.238, which was considered as a reasonable 