Scaling relations between several mass and structural properties of our galaxy samples. In the top row, (a) HI diameter versus exponential stellar scale radius (D_HI vs. R_D), (b) stellar mass versus HI mass (log M_* vs. log M_HI); in the bottom row, (c) total baryonic mass versus total dynamical mass enclosed in within 4 R_D (log M_b vs. log M_dyn), (d) stellar mass versus total dynamical mass (log M_* vs. log M_dyn), (e) dark matter core density versus core density (ρ₀ vs. R_c). In all plots, the regression fits for LSBs and dIrrs with their 68% (1-standard deviation) confidence intervals are shown in yellow and red, respectively, and the data for UDGs are superposed on their regression fits with teal stars. The R² values for the regression fit for LSBs and dIrrs (R_LSB² and R_dIrr², respectively) are mentioned at the bottom of each plot. Also, $\overline{p}$ and $\overline{\mathrm{AD}}$ are mentioned at the bottom of each plot, which measure the compliance of the UDG data with LSB or dIrr regression fit (${\overline{p}}_{\mathrm{LSB}}$, ${\overline{p}}_{\mathrm{dIrr}}$, ${\overline{\mathrm{AD}}}_{\mathrm{LSB}}$, and ${\overline{\mathrm{AD}}}_{\mathrm{dIrr}}$, respectively) obtained from the two-sample Anderson-Darling test. The steps of obtaining the $\overline{p}$ and $\overline{\mathrm{AD}}$ values are mentioned in Sect. 7.1.