The James Webb Space Telescope (JWST)/Mid-Infrared Instrument (MIRI) has revealed a large diversity of mid-infrared (mid-IR) spectral features from protoplanetary disks around faint very low-mass objects (VLMOs). The study of VLMO disks offers opportunities to investigate terrestrial planet formation as VLMOs are observed to host numbers of Earth to super-Earth planets. This study aims to quantify the chemical composition and abundances of dust in the surface layer of planet-forming disks around VLMOs observed by JWST/MIRI Medium Resolution Spectroscopy. We identify dust composition, constrain grain sizes, and summarize overall spectral trends. We measured the strength of the silicate band, the spectral slope of the Spectral Energy Distributions (SED), and the flux ratio of 13CCH2 and C2H2. We also performed retrieval modeling with the Dust Continuum Kit with Line emission from Gas to measure the mass fractions of silicate species and hydrocarbon lines that appear in mid-IR spectra. The strength of the silicate band is determined by the amount of micron-sized silicate dust in the disk surface. Thus, disks with strong silicate strength exhibit relatively low gas column densities because of high dust opacity. In addition, large silicate grains easily dominate the mass fraction in the disk surface. As a disk starts to settle, the larger dust grains settle first. Thus, the relative contribution of smaller grains to the mass fraction increases, and the silicate strength becomes weaker.