tokens: With that purpose, we have selected seven regions where the dust-to-gas ratio is larger than the mean expected value for the diffuse ISM, and for consistency, we keep the same names as in Paper I : H1, H2, H4, L1, L2, L4, and M1. In regions H1–H4, the gas density value ρ is greater than 1 σ ; in regions L1–L4, it is lower than 1 σ ; and in region M1, the gas density reaches intermediate values. In all cases, conspicuous filaments of charged dust are formed aligned with the magnetic fields. We want to note that the computational domains for coagulation simulations are squared domains that contain the original regions, so their limits are slightly different from those in Paper I ; the properties of these regions are summarized in Table 1 . Table 1 Properties of the Selected Regions Note. Regions selected from the turbulence simulation (Paper I ) to study the performance of the dust coagulation algorithm. In all cases, they are taken to be squared regions of a fixed length as given in the table, and with a uniform resolution in x - and y -directions. Given a region, we extract the gas properties and particle positions and set them inside a new domain with normalized limits [0, 1] × [0, 1]. The boundary conditions are outflow to ensure that the divergence-free constraint holds, ∇ · B = 0. This implies that some mass of dust will be inevitably lost, but we will take this fact into account when discussing the performance of the algorithm. The initial dust population is homogeneous, with a common radius of 0.05 μ m, a charge of Z d = −17, and an internal solid density . As explained in Section 2 , the computational test particles have to be considered as the centroids of a squared cloud with linear size 2 b that depends on the dust content. At the initial stage, all the clouds have the same linear size, typically 1.4 times the pixel size; this means that the clouds span a region of 2 × 2 pixels. The system is then left to evolve an arbitrary amount of time that differs from simulation to simulation. The final time is subjectively set following the condition that dust particles have moved enough to produce substantial coagulation, but they have not been completely swept away from the domain. A typical value is (∼3 × 10 −3 Myr; see Table 1 ), which, when compared with the global simulation (), is ∼7% of the total time. Hence, we expect that the phenomena observed in the simulations presented here are representative of the evolution of the global system (Paper I ) at short timescales. Besides, if we compare this time with the typical lifetime of a molecular cloud (∼10 6 Myr; Hartmann et al. 2001 ), it is evident that the timescales treated in this work are so small that we can consider that the final size distributions are representative for a molecular cloud at any stage of its evolution, provided that the ambient conditions (temperature, ionization fraction, magnetic field strength, and density) are maintained. 3.1. Evolution of the Size
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