Notes. ^(a) FWHM is measured with ATLASGAL870 μm continuum by Csengeri et al. (2014). r is derived from FWHM and distance but deconvolved with the beam of ATLASGAL image (19.2′′). See details in Yuan et al. (2017) and Paper I. ^(b)Distance is taken from Paper I. ^(c)Clump mass M_clump, H₂ column density , and dust temperature T_dust are derived by fitting SED pixel-by-pixel to Herschel 160, 250, 350, 500 μm, and ATLASGAL 870 μm by Yuan et al. (2017) but updated with the new distance by Paper I. ^(d) is the beam-averaged H₂ column density taken from SED fitting resulted maps with a beam of 36.4′′. ^(e) Surface density Σ is derived by the clump mass divided by π × r². The r is the deconvolved radius in the third column. ^(f) α is the power-law index of H₂ column density radial profile (r) ∝ r^α, see details in Paper I. ^(g)The FWHM line widths for the same pair of sources are taken from the same survey as possible as much. The abbreviation “S-C ¹⁸ O” means SEDIGISM C¹⁸O J = 2− 1 transition (Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium survey, Schuller et al. 2017). “F − ¹³ CO” and “F-C ¹⁸ O” represent FUGIN ¹³CO J = 1− 0 and C¹⁸ O J = 1−0 transitions, respectively (FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope, Umemoto et al. 2017). “H ¹³ CO⁺” is MALT90 H¹³ CO⁺ J = 1−0 transition (Millimetre Astronomy Legacy Team 90 GHz, Jackson et al. 2013).