Evolution of dust mass (black lines), planetesimal mass (red lines), and dust mass fraction within the pressure bump in three Stokes number bins (light blue for St<10⁻², blue for 10⁻² ≤ St ≤ 10⁻¹, and deep blue for St>10⁻¹), across four evolutionary stages: (i) pre-cavity, (ii) cavity at 10 au, (iii) cavity at 20 au, and (iv) cavity at 100 au. These panels show how initial conditions affect dust retention and planetesimal formation: Panel a: fiducial model (Z=0.01, L_X=2.6 L_{X, ⊙}, M_disk=0.05 M_⊙, R_c=60 au, α=10⁻⁴) serves as the baseline for comparison, showing balanced dust evolution and planetesimal production across the disk. Panel b: higher metallicity (Z=0.02) facilitates the retention of dust mass, thereby promoting planetesimal formation. Panel c: decreased X-ray luminosity (from 2.6 L_{X, ⊙} to 1.0 L_{X, ⊙}) diminishes dust mass and consequently impedes planetesimal formation. Panel d: higher viscosity parameters (α=10⁻³, δ_t=10⁻⁴) induce gas replenishment from the outer disk, delay cavity opening, reduce the overall dust reservoir, and thus hinder planetesimal formation. Panel e: a more massive and extended disk (M_disk=0.1 M_⊙, R_c=120 au) prolongs dust retention, thereby extending the duration of planetesimal formation. Panel f: a less massive but extended disk (M_disk=0.05 M_⊙, R_c=120 au) lowers the inner-disk dust density, causing photoevaporation to open a cavity earlier. This makes more dust retained at the onset of photoevaporative cavity, which also provides more building blocks for planetesimal formation.