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We have modified the iterative procedure introduced by Lin et al. (2016), tosystematically combine the submm images taken from ground based (e.g., CSO,JCMT, APEX) and space (e.g., Herschel, Planck) telescopes. We applied theupdated procedure to observations of three well studied Infrared Dark Clouds(IRDCs): G11.11-0.12, G14.225-0.506 and G28.34+0.06, and then performedsingle-component, modified black-body fits to derive $\sim$10$"$ resolutiondust temperature and column density maps. The derived column density maps showthat these three IRDCs exhibit complex filamentary structures embedding withrich clumps/cores. We compared the column density probability distributionfunctions (N-PDFs) and two-point correlation (2PT) functions of the columndensity field between these IRDCs with several OB cluster-forming regions.Based on the observed correlation and measurements, and complementaryhydrodynamical simulations for a 10$^{4}$ $\rm M_{\odot}$ molecular cloud, wehypothesize that cloud evolution can be better characterized by the evolutionof the (column) density distribution function and the relative power of densestructures as a function of spatial scales, rather than merely based on thepresence of star-forming activity. Based on the small analyzed sample, wepropose four evolutionary stages, namely: {\it cloud integration, stellarassembly, cloud pre-dispersal and dispersed-cloud.} The initial {\it cloudintegration} stage and the final {\it dispersed cloud} stage may bedistinguished from the two intermediate stages by a steeper than $-$4 power-lawindex of the N-PDF. The {\it cloud integration} stage and the subsequent {\itstellar assembly} stage are further distinguished from each other by the largerluminosity-to-mass ratio ($>$40 $\rm L_{\odot}/M_{\odot}$) of the latter.

Cloud structure of three Galactic infrared dark star-forming regions from combining ground and space based bolometric observations